DOCSLIB.ORG

Parker Solar Probe SWG Telecon February 5, 2020 Project Science Report Nour Raouafi Project Status Helene Winters Payload Status SB,JK,DM,RH Solar Orbiter H

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Parker Solar Probe SWG Telecon February 5, 2020 Project Science Report Nour Raouafi Project Status Helene Winters Payload Status SB,JK,DM,RH Solar Orbiter H Parker Solar Probe SWG Telecon February 5, 2020 Project Science Report Nour Raouafi Project Status Helene Winters Payload Status SB,JK,DM,RH Solar Orbiter H. Gilbert/C. St. Cyr SOC Activities Martha Kusterer Payload SE Telecon S. Hamilton/A. Reiter Theory Group M. Velli/A. Higginson Upcoming Meetings Nour Raouafi Science Presentations: DaviD Malaspina (LASP) & Karl Battams (NRL) Agenda • DCP 5 Information • DCP Type: Data Volume • Venus Flyby • Non-routine Activities & Science Priorities o WISPR o ISOIS o FIELDS o SWEAP • Modeling – Robert Allen • Coordinated observations. Parker Solar Probe Project Science SWG Telecon February 5, 2020 ApJS Special Issue (ApJ/SI) 50+ papers submitted as of Oct. 20, 2019 Early Results from Parker Solar Probe: Ushering a New Frontier in Space Exploration • Publication Date: February 3, 2020 • 48 papers accessible online • Few more papers still under review Corresponding authors: please speed up the reviewing process – Send me your submission info and the manuscript. • Print copies: Science Teams are you interested in ordering print copies of the special issue? 2/7/20 4 Nature Papers ADS not listing all the authors • ADS lists only three authors: the first two and the last one • The issue was addressed for the FIELDS and WISPR papers • But not for the SWEAP and ISOIS papers • ADS stated that that’s the information Nature sent to them • Corrections can submitted through http://adsabs.harvard.edu/adsfeedback/submit_abstract.php. 2/7/20 5 Future Publications • Let’s us know about your results in case we need to prepare for press releases • Animations take time to design and get ready • Please do not for the mission acknowledgements Parker Solar Probe was designed, built, and is now operated by the Johns Hopkins Applied Physics Laboratory as part of NASA’s Living with a Star (LWS) program (contract NNN06AA01C). Support from the LWS management and technical team has played a critical role in the success of the Parker Solar Probe mission. 2/7/20 6 Parker One March 23-27, 2020 • 182 abstract submitted so far • Submission will remain open for late abstracts • ~150 attendees registered If you have not registered yet, please consider to do so soon • Hotels, info website Parker One Science Program • Science Organizing Committee: Marco Velli (Co-Chair), Nicholeen Viall (Co-Chair), Stuart Bale, Benjamin Chandran, Christina Cohen, Rob Decker, Aleida Higginson, Russell Howard, Colin Joyce, Justin Kasper, David Lario, David J. McComas, Nour E. Raouafi, Adam Szabo, Anna Tenerani, Angelos Vourlidas • 13 Invited talks • 40 Contributed talks • Two poster sessions, ~70 posters each 1st session: Monday-Tuesday 2nd session: Wednesday-Thursday • Data tutorials Marc Pulupa (FIELDS) Tony Case (SWEAP) Nathan Schwadron (ISOIS) Guillermo Stenborg (WISPR) Space- and Ground-based Support Encounter 4 and beyond ~50 observatories around the globe support Parker Enc. 4 • Space: Hinode, IRIS, SDO, STEREO, NuSTAR, MMS, … • Ground: >40 observatories • Modeling: 7 teams provide predictions of the SC B- connectivity Data distribution: Space- and Ground-based Support Leads PSP E4: Ground-Based Optical Solar Observatories Observatory Location/Time Observations POC Mauna Loa Solar Observatory Big Island of • White light polarization brightness (pB) Joan Burkepile (MLSO) Hawaii, USA • Coronal electron densities 19.5°N • 15s cadence 155.6°W Daily (1700- 0200UT) Big Bear Solar Observatory California, USA • Imaging spectroscopy and polarimetry Wedna Cao (BBSO) Daily • 0.1” resolution Haimin Wang Dunn Solar Telescope New Mexico, • Imaging and spectroscopy at multiple wavelengths Damian Christian USA • IR spectro-polarimetry Jan 15-31 (1500-1700UT) Sayan Solar Obbservatory Russia • Spectrograms and vector magnetograms Misha Demidov 51.6°N 108°E • Coronal obbservations Daily Baikal Astrophysical Russia • Call K Misha Demidov Observatory 54.8°N 105°E • Magnetic Field Daily Kislovodsk Observatory Russia • Full-disk Call K and Halpha (1m cadence) Andrey Tlatov 43.7°N 42.3°E • Photospheric magnetograms2/7/20 Support for PSP Encounter 4 | SPWG Telecon 11 PSP E4: Ground-Based Optical Solar Observatories Observatory Location/Time Observations POC Fuxian Solar Observatory China • High-res 0.3” Halpha images with 11s cadence Zhi Xu 1m NVST telescope 24.6°N 103°E • High-res ~0.1” (after reconstruction) images in the TiO band 0100-0800UT with 30s cadence Huairou Solar Observing China • Halpha Xianyong Bai Station (HSOS) 40.4°N 116.6°E • Photospheric vector magnetic fields 0030-0830UT • Chromospheric LOS magnetic fields ONSET Telescope China Pengfei Chen Istituto Ricerche Solari Locarno, • High-precision polarimetry in the Cal 422.7 nm limb (both limb Renzo Ramelli Locarno (IRSOL) Switzerland and disk) Michele Bianda 46.2°N 8.8°E • Other possible lines include: Na I D1 and D2, He D3, H-alpha, and a C2 molecular band Kanzelhöhe Observatory Austria • Full-disk images in Halpha, Call K, and white light Werner Pötzi 46.7°N 13.9°E • 10 images/minute (4 images/s in flare mode) Daily Hvar Observatory Zagreb, Croatia • Halpha and white light high cadence 2s images Jasa Calogovic 43.2°N 16.5°E • FOV 7 and 11 arcmin, 1” spatial resolution 0600-1300UT 2/7/20 Support for PSP Encounter 4 | SPWG Telecon 12 PSP E4: Ground-Based Optical Solar Observatories Observatory Location/Time Observations POC Astronomical Observatory of Monte Porzio • Full-disk Call K, G-band, res and blue cont. Ilaria Ermolli Rome (PSPT) Catone, Rome, • ~2” resolution, 0.1% pixel-to-pixel precision Italy Catania Solar Observatory Catania, Sicily, • Full-disk images in Halpha and cont at 656nm Paolo Romano Italy • 2” spatial resolution 37.5°N 15.1°E • 1m cadence in campaign mode Pic du Midi Pyrenees, FR • Coronagraphic observations in Halpha and Hel, possibly in Fe Frederic Pitout 42.9°N 0.1°E XII 1074 nm Arturo Lopez Ariste Meudon Observatory France • Full disk Halpha Jean-Marie Malherbe 48.8°N 2.3°E Daily NSO/GONG Netword Multiple • High-sensitivity magnetograms, velocity and intensity images at Alexei Pevtsov locations 1m cadence ~90% duty • Near-real-time seismic images of the farside cycle • Halpha images at 20s cadence Mitaka Observatory Japan • Full-disk Halpha, G-band, Call K, cont. Yoichiro Hanaoka • Halpha velocity maps • Full-disk magnetograms in He 10830Å, Si 10827Å, and Fe 15648Å 2/7/20 Support for PSP Encounter 4 | SPWG Telecon 13 PSP E4: Ground-Based Optical Solar Observatories Observatory Location/Time Observations POC Hida Observatory Japan • Full-disk Halpha images Kiyoshi Ichimoto Félix Aguilar Observatory Argentina • Full-disk H-alpha center line with a 1m cadence Carlos Francile 31.8°S 69.3°W • 30 THz camera (70% of the disk) with 1s cadence Latin America Giant Marambio, • Cosmic rays 2-100 GeV Sergio Dasso Observaory (LAGO)/NEWRUS Antartica 64°S 57°W (etc) Crimean Astrophysical Crimea • Monochromatic and spectral images Valentina Abramenko Observatory (CrAO) 2/7/20 Support for PSP Encounter 4 | SPWG Telecon 14 PSP E4: Ground-Based Radio Solar Observatories Observatory Location/Time Observations POC Arecibo Mike Sulzer [email protected] Expanded Owens Walley California, USA • Microwave spectra and iMaging 1-18GHz Dale Gary Solar Array (EOVSA) Daily (1600- • Full-disk iMages 1/day at 6 frequency bands Sherry Chhabbra 2400UT) • Full-Sun-integrated spectrograMs, 1s cadence Bin Chen Very Large Array (VLA) New Mexico, • Imaging at 1-2 GHz & 230-470 MHz TiM Bastian USA Jan 28, 30, 31 (TBC) Jan 27 • Full-disk Mosaic L & S band Stephen White Long Wavelength Array New Mexico, • 20-80 MHz spectroscopy Stephen White (LWA) USA Jan 27-30 (TBC) NobeyaMa Radioheliograph Japan • Full-disk iMages at 17 and 34 GHz Satoshi Masuda 2300-0600 UT Kislovodsk Observatory Russia • Radio observations at 3 and 5cM Andrey Tlatov 43.7°N 42.3°E MeerKAT South Africa Du Toit 2/7/20 SupportJaMes for PSP Chibueze Encounter 4 | SPWG Telecon 15 PSP E4: Ground-Based Radio Solar Observatories Observatory Location/Time Observations POC Siberian Radioheliograph Siberia, Russia • Full-disk images at 16 or 32 bands in 4-8 GHz range Maria Globa 51.8°N 103°E Alexander Altyntsev Daily 0200- Sergey Lesovoi 0800UT Huairou Solar Radio China Baolin Tan Spectrograph Low-Frequency Array (LOFAR) Netherlands • Solar imaging range 20-70MHz Richard Fallows • High-res solar dynamic spectra 10-77MHz and 110-190MHz Pietro Zucca Murchison Widefield Array Austrailia • Imaging spectroscopy at 24 bands 80-240 MHz Divya Oberoi • 0.5s and 40 kHz resolution Sardinia Radio Telescope San Basilio, • Full-disk solar images at 18 and 26 GHz Alberto Pellizzoni (SRT) Sardinia, Italy • ~50” arcsec angular res 39.5°N 9.2°E Jan 28 0800- 1500UT Nançay Decameter Array France • 10-100 MHz daily spectrograms of the Sun and Jupiter at Sophie Masson 47.4°N 2.2°E various cadences (<1s) and spectral resolutions (<175 kHz) Laurent Lamy Daily 2/7/20 Support for PSP Encounter 4 | SPWG Telecon 16 PSP E4: Ground-based Geospace Observatories Observatory/Satellite Observing Observations POC Mission Window PFISR Continuous • IPY27 (1% duty cycle): 4 beams, long pulse (F-region) and Roger Varney (low duty cycle) alternating codes (E-region) [email protected] • Themis36: 23 beams, long pulse (F-region) and alternating codes (E-region) • MSWinds26 (For ELFIN): 4 beams, barker codes (D-region), alternating codes (E-region), and long pulse (F-region) • WorldDay35: 11 beams, long pulse (F-region) and alternating codes (E-region) Calendar: data.amisr.com/database/61/sched/2020/01/ RISR-N Continuous • LowDuty2 (3.5% duty cycle): 5 beams long pulse (F-region) and Roger
Load more

Recommended publications
  • Exhibits and Financial Statement Schedules 149
    Table of Contents UNITED STATES SECURITIES AND EXCHANGE COMMISSION Washington, D.C. 20549 FORM 10-K [ X] ANNUAL REPORT PURSUANT TO SECTION 13 OR 15(d) OF THE SECURITIES EXCHANGE ACT OF 1934 For the fiscal year ended December 31, 2011 OR [ ] TRANSITION REPORT PURSUANT TO SECTION 13 OR 15(d) OF THE SECURITIES EXCHANGE ACT OF 1934 For the transition period from to Commission File Number 1-16417 NUSTAR ENERGY L.P. (Exact name of registrant as specified in its charter) Delaware 74-2956831 (State or other jurisdiction of (I.R.S. Employer incorporation or organization) Identification No.) 2330 North Loop 1604 West 78248 San Antonio, Texas (Zip Code) (Address of principal executive offices) Registrant’s telephone number, including area code (210) 918-2000 Securities registered pursuant to Section 12(b) of the Act: Common units representing partnership interests listed on the New York Stock Exchange. Securities registered pursuant to 12(g) of the Act: None. Indicate by check mark if the registrant is a well-known seasoned issuer, as defined in Rule 405 of the Securities Act. Yes [X] No [ ] Indicate by check mark if the registrant is not required to file reports pursuant to Section 13 or Section 15(d) of the Act. Yes [ ] No [X] Indicate by check mark whether the registrant (1) has filed all reports required to be filed by Section 13 or 15(d) of the Securities Exchange Act of 1934 during the preceding 12 months (or for such shorter period that the registrant was required to file such reports), and (2) has been subject to such filing requirements for the past 90 days.
    [Show full text]
  • Mission to Jupiter
    This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines.
    [Show full text]
  • Comet Lemmon, Now in STEREO 25 April 2013, by David Dickinson
    Comet Lemmon, Now in STEREO 25 April 2013, by David Dickinson heads northward through the constellation Pisces. NASA's twin Solar TErrestrial RElations Observatory (STEREO) spacecraft often catch sungrazing comets as they observe the Sun. Known as STEREO A (Ahead) & STEREO B (Behind), these observatories are positioned in Earth leading and trailing orbits. This provides researchers with full 360 degree coverage of the Sun. Launched in 2006, STEREO also gives us a unique perspective to spy incoming sungrazing comets. Recently, STEREO also caught Comet 2011 L4 PanSTARRS and the Earth as the pair slid into view. Another solar observing spacecraft, the European Space Agencies' SOlar Heliospheric Observatory (SOHO) has been a prolific comet discoverer. Amateur comet sleuths often catch new Kreutz group sungrazers in the act. Thus far, SOHO has Animation of Comet 2012 F6 Lemmon as seen from discovered over 2400 comets since its launch in NASA’s STEREO Ahead spacecraft. Credit: 1995. SOHO won't see PanSTARRS or Lemmon in NASA/GSFC; animation created by Robert Kaufman its LASCO C3 camera but will catch a glimpse of Comet 2012 S1 ISON as it nears the Sun late this coming November. An icy interloper was in the sights of a NASA Like SOHO and NASA's Solar Dynamics spacecraft this past weekend. Comet 2012 F6 Observatory, data from the twin STEREO Lemmon passed through the field of view of spacecraft is available for daily perusal on their NASA's HI2A camera as seen from its solar website. We first saw this past weekend's observing STEREO Ahead spacecraft. As seen in animation of Comet Lemmon passing through the animation above put together by Robert STEREO's field of view on the Yahoo Kaufman, Comet Lemmon is now displaying a fine STEREOHunters message board.
    [Show full text]
  • In-Flight PSF Calibration of the Nustar Hard X-Ray Optics
    In-flight PSF calibration of the NuSTAR hard X-ray optics Hongjun Ana, Kristin K. Madsenb, Niels J. Westergaardc, Steven E. Boggsd, Finn E. Christensenc, William W. Craigd,e, Charles J. Haileyf, Fiona A. Harrisonb, Daniel K. Sterng, William W. Zhangh aDepartment of Physics, McGill University, Montreal, Quebec, H3A 2T8, Canada; bCahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA; cDTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark; dSpace Sciences Laboratory, University of California, Berkeley, CA 94720, USA; eLawrence Livermore National Laboratory, Livermore, CA 94550, USA; fColumbia Astrophysics Laboratory, Columbia University, New York NY 10027, USA; gJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA; hGoddard Space Flight Center, Greenbelt, MD 20771, USA ABSTRACT We present results of the point spread function (PSF) calibration of the hard X-ray optics of the Nuclear Spectroscopic Telescope Array (NuSTAR). Immediately post-launch, NuSTAR has observed bright point sources such as Cyg X-1, Vela X-1, and Her X-1 for the PSF calibration. We use the point source observations taken at several off-axis angles together with a ray-trace model to characterize the in-orbit angular response, and find that the ray-trace model alone does not fit the observed event distributions and applying empirical corrections to the ray-trace model improves the fit significantly. We describe the corrections applied to the ray-trace model and show that the uncertainties in the enclosed energy fraction (EEF) of the new PSF model is ∼<3% for extraction ′′ apertures of R ∼> 60 with no significant energy dependence.
    [Show full text]
  • Building Nustar's Mirrors
    20 | ASK MAGAZINE | STORY Title BY BUILDING NUSTAR’S MIRRORS Intro Many NASA projects involve designing and building one-of-a-kind spacecraft and instruments. Created for particular, unique missions, they are custom-made, more like works of technological art than manufactured objects. Occasionally, a mission calls for two identical satellites (STEREO, the Solar Terrestrial Relations Observatory, for instance). Sometimes multiple parts of an instrument are nearly identical: the eighteen hexagonal beryllium mirror segments that will form the James Webb Space Telescope’s mirror are one example. But none of this is mass production or anything close to it. nn GuisrCh/ASA N:tide CrothoP N:tide GuisrCh/ASA nn Niko Stergiou, a contractor at Goddard Space Flight Center, helped manufacture the 9,000 mirror segments that make up the optics unit in the NuSTAR mission. ASK MAGAZINE | 21 BY WILLIAM W. ZHANG The mirror segments my group has built for NuSTAR, the the interior surface and a bakeout, dries into a smooth and clean Nuclear Spectroscopic Telescope Array, are not mass produced surface, very much like glazed ceramic tiles. Finally we had to either, but we make them on a scale that may be unique at NASA: map the temperatures inside each oven to ensure they would we created more than 20,000 mirror segments over a period of two provide a uniform heating environment so the glass sheets years. In other words, we’re talking about some middle ground could slump in a controlled and gradual way. Any “wrinkles” between one-of-a-kind custom work and industrial production.
    [Show full text]
  • Nustar Observatory Guide
    NuSTAR Guest Observer Program NuSTAR Observatory Guide Version 3.2 (June 2016) NuSTAR Science Operations Center, California Institute of Technology, Pasadena, CA NASA Goddard Spaceflight Center, Greenbelt, MD nustar.caltech.edu heasarc.gsfc.nasa.gov/docs/nustar/index.html i Revision History Revision Date Editor Comments D1,2,3 2014-08-01 NuSTAR SOC Initial draft 1.0 2014-08-15 NuSTAR GOF Release for AO-1 Addition of more information about CZT 2.0 2014-10-30 NuSTAR SOC detectors in section 3. 3.0 2015-09-24 NuSTAR SOC Update to section 4 for release of AO-2 Update for NuSTARDAS v1.6.0 release 3.1 2016-05-10 NuSTAR SOC (nusplitsc, Section 5) 3.2 2016-06-15 NuSTAR SOC Adjustment to section 9 ii Table of Contents Revision History ......................................................................................................................................................... ii 1. INTRODUCTION ................................................................................................................................................... 1 1.1 NuSTAR Program Organization ..................................................................................................................................................................................... 1 2. The NuSTAR observatory .................................................................................................................................... 2 2.1 NuSTAR Performance ........................................................................................................................................................................................................
    [Show full text]
  • The Explorer Program
    The Explorer Program Presentation to the Astrophysics Subcommittee Wilton Sanders Explorer Program Scientist Astrophysics Division NASA Science Mission Directorate November 19, 2013 1 Astrophysics Explorer Program • The Astrophysics and the Heliophysics Explorer Programs are separate. • Current Astrophysics Explorer Missions: - Operating (and will be included in the 2014 Senior Review) • Swift (MIDEX), launched 2004 November 20 • Suzaku (MO – partnered with JAXA), launched 2005 July 10 • NuSTAR (SMEX), launched 2012 June 13 - In Development • ASTRO-H (MO – partnered with JAXA), scheduled for launch in 2015 - In Formulation • NICER (MO), targeted for transportation to ISS in 2016 • TESS (EX), targeted for launch in 2017 • Future AOs - SMEX and MO in late summer/early fall 2014 for launch ~ 2020 - EX and MO NET 2016 for launch ~ 2022 2 2014 Astrophysics Explorer AO • Community Announcement released on 2013 November 12 that NASA will solicit proposals for SMEX missions and Missions of Opportunity. • Draft AO targeted for spring 2014, with Explorer Workshop ~ 2 weeks later. • Final AO targeted for late summer/early fall 2014, with Pre-Proposal Conference ~ 3 weeks after final AO release. Proposals due 90 days after AO release. • PI cost cap $125M (FY2015$) for SMEX, not including cost of ELV or transportation to the ISS. • MOs allowed in all three categories: Partner MO, New Missions using Existing Spacecraft, or Small Complete Mission, including those requiring flight on the ISS. • PI cost cap $35M for sub-orbital class MOs, which include ultra-long duration balloons, suborbital reusable launch vehicles, and CubeSats. Other MOs (not suborbital-class) have a $65M PI cost cap. • Two-step process.
    [Show full text]
  • Activity - Sunspot Tracking
    JOURNEY TO THE SUN WITH THE NATIONAL SOLAR OBSERVATORY Activity - SunSpot trAcking Adapted by NSO from NASA and the European Space Agency (ESA). https://sohowww.nascom.nasa.gov/classroom/docs/Spotexerweb.pdf / Retrieved on 01/23/18. Objectives In this activity, students determine the rate of the Sun’s rotation by tracking and analyzing real solar data over a period of 7 days. Materials □ Student activity sheet □ Calculator □ Pen or pencil bacKgrOund In this activity, you’ll observe and track sunspots across the Sun, using real images from the National Solar Observatory’s: Global Oscillation Network Group (GONG). This can also be completed with data students gather using www.helioviewer.org. See lesson 4 for instructions. GONG uses specialized telescope cameras to observe diferent layers of the Sun in diferent wavelengths of light. Each layer has a diferent story to tell. For example, the chromosphere is a layer in the lower solar atmosphere. Scientists observe this layer in H-alpha light (656.28nm) to study features such as flaments and prominences, which are clearly visible in the chromosphere. For the best view of sunspots, GONG looks to the photosphere. The photosphere is the lowest layer of the Sun’s atmosphere. It’s the layer that we consider to be the “surface” of the Sun. It’s the visible portion of the Sun that most people are familiar with. In order to best observe sunspots, scientists use photospheric light with a wavelength of 676.8nm. The images that you will analyze in this activity are of the solar photosphere. The data gathered in this activity will allow you to determine the rate of the Sun’s rotation.
    [Show full text]
  • Observational Artifacts of Nustar: Ghost-Rays and Stray-Light
    Observational Artifacts of NuSTAR: Ghost-rays and Stray-light Kristin K. Madsena, Finn E. Christensenb, William W. Craigc, Karl W. Forstera, Brian W. Grefenstettea, Fiona A. Harrisona, Hiromasa Miyasakaa, and Vikram Ranaa aCalifornia Institute of Technology, 1200 E. California Blvd, Pasadena, USA bDTU Space, National Space Institute, Technical University of Denmark, Elektronvej 327, DK-2800 Lyngby, Denmark cSpace Sciences Laboratory, University of California, Berkeley, CA 94720, USA ABSTRACT The Nuclear Spectroscopic Telescope Array (NuSTAR), launched in June 2012, flies two conical approximation Wolter-I mirrors at the end of a 10.15 m mast. The optics are coated with multilayers of Pt/C and W/Si that operate from 3{80 keV. Since the optical path is not shrouded, aperture stops are used to limit the field of view from background and sources outside the field of view. However, there is still a sliver of sky (∼1.0{4.0◦) where photons may bypass the optics altogether and fall directly on the detector array. We term these photons Stray-light. Additionally, there are also photons that do not undergo the focused double reflections in the optics and we term these Ghost Rays. We present detailed analysis and characterization of these two components and discuss how they impact observations. Finally, we discuss how they could have been prevented and should be in future observatories. Keywords: NuSTAR, Optics, Satellite 1. INTRODUCTION 1 arXiv:1711.02719v1 [astro-ph.IM] 7 Nov 2017 The Nuclear Spectroscopic Telescope Array (NuSTAR), launched in June 2012, is a focusing X-ray observatory operating in the energy range 3{80 keV.
    [Show full text]
  • Collision Avoidance Operations in a Multi-Mission Environment
    AIAA 2014-1745 SpaceOps Conferences 5-9 May 2014, Pasadena, CA Proceedings of the 2014 SpaceOps Conference, SpaceOps 2014 Conference Pasadena, CA, USA, May 5-9, 2014, Paper DRAFT ONLY AIAA 2014-1745. Collision Avoidance Operations in a Multi-Mission Environment Manfred Bester,1 Bryce Roberts,2 Mark Lewis,3 Jeremy Thorsness,4 Gregory Picard,5 Sabine Frey,6 Daniel Cosgrove,7 Jeffrey Marchese,8 Aaron Burgart,9 and William Craig10 Space Sciences Laboratory, University of California, Berkeley, CA 94720-7450 With the increasing number of manmade object orbiting Earth, the probability for close encounters or on-orbit collisions is of great concern to spacecraft operators. The presence of debris clouds from various disintegration events amplifies these concerns, especially in low- Earth orbits. The University of California, Berkeley currently operates seven NASA spacecraft in various orbit regimes around the Earth and the Moon, and actively participates in collision avoidance operations. NASA Goddard Space Flight Center and the Jet Propulsion Laboratory provide conjunction analyses. In two cases, collision avoidance operations were executed to reduce the risks of on-orbit collisions. With one of the Earth orbiting THEMIS spacecraft, a small thrust maneuver was executed to increase the miss distance for a predicted close conjunction. For the NuSTAR observatory, an attitude maneuver was executed to minimize the cross section with respect to a particular conjunction geometry. Operations for these two events are presented as case studies. A number of experiences and lessons learned are included. Nomenclature dLong = geographic longitude increment ΔV = change in velocity dZgeo = geostationary orbit crossing distance increment i = inclination Pc = probability of collision R = geostationary radius RE = Earth radius σ = standard deviation Zgeo = geostationary orbit crossing distance I.
    [Show full text]
  • Astrophysics
    National Aeronautics and Space Administration Astrophysics Committee on NASA Science Paul Hertz Mission Extensions Director, Astrophysics Division NRC Keck Center Science Mission Directorate Washington DC @PHertzNASA February 1-2, 2016 Why Astrophysics? Astrophysics is humankind’s scientific endeavor to understand the universe and our place in it. 1. How did our universe 2. How did galaxies, stars, 3. Are We Alone? begin and evolve? and planets come to be? These national strategic drivers are enduring 1972 1982 1991 2001 2010 2 Astrophysics Driving Documents http://science.nasa.gov/astrophysics/documents 3 Astrophysics Programs Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program 1. How did our universe 2. How did galaxies, stars, 3. Are We Alone? begin and evolve? and planets come to be? Astrophysics Explorers Program Astrophysics Research Program James Webb Space Telescope Program (managed outside of Astrophysics Division until commissioning) 4 Astrophysics Programs and Missions Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program Chandra Hubble Spitzer Kepler/K2 XMM-Newton (ESA) Herschel (ESA) WFIRST Fermi SOFIA Planck (ESA) LISA Pathfinder (ESA) Astrophysics Explorers Program Euclid (ESA) NuSTAR Swift Suzaku (JAXA) Athena (ESA) ASTRO-H (JAXA) NICER TESS L3 GW Obs (ESA) 3 SMEX and 2 MO in Phase A James Webb Space Telescope Program: Webb 5 Astrophysics Programs and Missions Physics of the Cosmos Cosmic Origins Exoplanet Exploration Program Program Program Missions in extended phase Chandra Hubble Spitzer Kepler/K2 XMM-Newton (ESA) Herschel (ESA) WFIRST Fermi SOFIA Planck (ESA) LISA Pathfinder (ESA) Astrophysics Explorers Program Euclid (ESA) NuSTAR Swift Suzaku (JAXA) Athena (ESA) ASTRO-H (JAXA) NICER TESS L3 GW Obs (ESA) 3 SMEX and 2 MO in Phase A James Webb Space Telescope Program: Webb 6 Astrophysics Mission Portfolio • NASA Astrophysics seeks to advance NASA’s strategic objectives in astrophysics as well as the science priorities of the Decadal Survey in Astronomy and Astrophysics.
    [Show full text]
  • Ground-Based Solar Physics in the Era of Space Astronomy a White Paper Submitted to the 2012 Heliophysics Decadal Survey
    Ground-Based Solar Physics in the Era of Space Astronomy A White Paper Submitted to the 2012 Heliophysics Decadal Survey T. Ayres1, D. Longcope2 (on behalf of the 2009 AURA Solar Decadal Committee) Chromosphere-Corona at eclipse Hα filtergram Photospheric spots & bright points Same area in chromospheric Ca+ 1Center for Astrophysics and Space Astronomy, 389 UCB, University of Colorado, Boulder, CO 80309; [email protected] (corresponding author) 2Montana State University SUMMARY. A report, previously commissioned by AURA to support advocacy efforts in advance of the Astro2010 Decadal Survey, reached a series of conclusions concerning the future of ground-based solar physics that are relevant to the counterpart Heliophysics Survey. The main findings: (1) The Advanced Technology Solar Telescope (ATST) will continue U.S. leadership in large aperture, high-resolution ground-based solar observations, and will be a unique and powerful complement to space-borne solar instruments; (2) Full-Sun measurements by existing synoptic facilities, and new initiatives such as the Coronal Solar Magnetism Observatory (COSMO) and the Frequency Agile Solar Radiotelescope (FASR), will balance the narrow field of view captured by ATST, and are essential for the study of transient phenomena; (3) Sustaining, and further developing, synoptic observations is vital as well to helioseismology, solar cycle studies, and Space Weather prediction; (4) Support of advanced instrumentation and seeing compensation techniques for the ATST, and other solar telescopes, is necessary to keep ground-based solar physics at the cutting edge; and (5) Effective planning for ground-based facilities requires consideration of the synergies achieved by coordination with space-based observatories.
    [Show full text]